Spectral types and projected equatorial rotational velocities (vsini)
are determined, and standard photospheric stellar templates are
subtracted from the Ae/Be stellar spectra. The
residual spectra are then used to examine the
following accretion diagnostics: (1) the frequency of direct mass
inflow signatures as exhibited by inverse P-Cygni line profiles,
(2) relations between Balmer and forbidden line emission
and infrared color indices, (3) limits on any
optical continuum excess, or spectral ``veiling", which,
if produced in a hot boundary layer, sets limits on mass accretion rates.